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Modelling of massive stars and supernovae (SNe) plays a crucial role inunderstanding galaxies. From this modelling we can derive fundamentalconstraints on stellar evolution, mass-loss processes, mixing, and the productsof nucleosynthesis. Proper account must be taken of all important processesthat populate and depopulate the levels (collisional excitation, de-excitation,ionization, recombination, photoionization, bound-bound processes). For theanalysis of Type Ia SNe and core collapse SNe (Types Ib, Ic and II) Fe groupelements are particularly important. Unfortunately little data is currentlyavailable and most noticeably absent are the photoionization cross-sections forthe Fe-peaks which have high abundances in SNe. Important interactions for bothphotoionization and electron-impact excitation are calculated using therelativistic Dirac Atomic $R$-matrix Codes (DARC) for low ionization stages ofcobalt. All results are calculated up to photon energies of 45 eV and electronenergies up to 20 eV. The wavefunction representation of Co III has beengenerated using GRASP0 by including the dominant 3d$^7$, 3d$^6$[4s, 4p],3p$^4$3d$^9$ and 3p$^6$3d$^9$ configurations, resulting in 292 fine structurelevels. Electron-impact collision strengths and Maxwellian averaged effectivecollision strengths across a wide range of astrophysically relevanttemperatures are computed for Co III. In addition, statistically weightedlevel-resolved ground and metastable photoionization cross-sections arepresented for Co II and compared directly with existing work.

Photoionization of Co$^{+}$ and electron-impact excitation of Co$^{2+}$ using the Dirac R-matrix method